PPT-WFC3 slitless spectroscopy

Harald Kuntschner Martin Kümmel Jeremy Walsh STECF Howard Bushouse STScI Grism Workshop STScI November 15 2010 WFC3 UV Channel IR Channel Filter wheels with WFC3 grisms. . C. luster . L. ensing . A. nd . S. upernova survey with . H. ubble. ACS Parallels. WFC3 Parallels. 6 arcmin. = 2.2 Mpc @ z=0.5. Footprints of HST Cameras: . ACS FOV in yellow, . WFC3/IR FOV in red, . An Innovative. Multi-cycle Hubble Treasury Program to . Study the Dark Universe. Marc . Postman. Space Telescope Science . Institute. Science with HST III, Venice, Italy. October 2010. MACS 2129-0741 z = 0.57 HST/ACS image (. Spectr. . scopy. with NIRISS. Van Dixon. STScI. JWST FGS. TIPS/JIM. 2012 September 20. . NIRISS at a Glance. Parameter. Value. Array Size. 2048 x 2048 (2040 x 2040 active). Pixel size. 18 . μm. x 18 . Outline. 1.) Step 1 – TV3 Calibration. 2.) Step 2 – SMOV4 (+ Cycle 17 Calibration). 3.) Step 3 – Final Calibration (present analysis). - More data. - New flat fields. - Astrodrizzle. - Precise calibration. Acknowledgments. Zach . Berta (Harvard), the P.I. of HST program 12251, “The first characterization of a Super-Earth Atmosphere,” graciously agreed to our request to use GJ 1214 also for our engineering test, program 12325. Many persons, especially Merle Reinhart, Alan Welty, and William “Bill” Januszewski (STScI) helped plan the observations. Art Bradley (SSES) and Mike Wenz (GSFC) provided FGS data and analysis. . Redshift. Galaxies . in Cluster Fields. Wei Zheng, Larry Bradley, and the CLASH high-. z. search group. High-Redshift Galaxies. Key Science Questions:. How do the first generations of galaxies build up and evolve at the earliest times?. Exoplanets. ). STScI. Calibration Workshop. Aug 13, 2014. Peter R. McCullough. H. 2. O. H. 2. O. 0. th . order. 1. st . order. 2. nd . order. Spatially Scanned (vertically). Staring Mode (nominal). . An Innovative. Multi-cycle Hubble Treasury Program to . Study the Dark Universe. Marc . Postman. Space Telescope Science . Institute. Science with HST III, Venice, Italy. October 2010. MACS 2129-0741 z = 0.57 HST/ACS image (. Lo. ïc Albert (with help from Étienne, David and Jason). Science Team Meeting. UdeM, October 20 2015. Simulation Objectives. Test different trace extraction. scenarios to devise an optimal extraction method and calibration strategy.. Fall . 2017. First Order Spectra. For a spectrum to be 1. st. order, the . D. n. between the chemical shifts of any given pair of nuclei must be much larger than the value of the coupling constant . Piet Van Duppen. ISOLDE CERN, Switzerland. IKS-. K.U.Leuven. , Belgium. K.U. Leuven. University of Western Scotland, U.K. - . K.U.Leuven. , Belgium - SCK-CEN-Mol, Belgium - . U.Gent. , Belgium - . Commenius. on behalf of the MIRI Team. MIRI Low Resolution Spectroscopy. Low-resolution Spectroscopy Overview. Design and operating principles. Focal plane locations. LRS testing & data. Preparing an LRS observation: slit vs. slitless. 2. Nuclear Magnetic Resonance Spectroscopy. After hydrogen, the most useful atom providing information is carbon-13.. The . overall intensity of a . 13. C signal is about 6400 . times . less than the intensity of an . William Frost. MSc - . UdeM. In collaboration with. Loïc Albert, . Ren. é Doyon & Björn . Benneke. Summary of Research. Construct an emission spectrum of a brown dwarf (BD) from existing observations.